In this paper we will consider three reddening curves. The first is a typical Milky Way reddening curve, as parametrized by [1]}. A Milky Way curve has long been ruled out for the majority of AGNs because they do not show the strong \(\) 2175 dust feature, so we are only including the Milky Way curve for comparison. We then consider two reddening curves proposed for AGNs: the mean AGN reddening curve given by [2]}, and an SMC-like curve as parametrized by [1]}. [2]} only gave their mean AGN curve for wavelengths from Lyman \(\)  to H\(\) , but we consider Paschen \(\)  here as well. Since the SMC and Milky Way curves are similar from H\(\)  to Pa\(\) , we have extended the Gaskell & Benker curve to longer wavelengths by taking the average of the Milky Way and SMC curves.
Table 1 summarizes our adopted factors for the three reddening curves for converting \(E(_1-_2)\)  to \(E(B-V)\)  for the pairs of wavelengths we consider (i.e., the right hand side of Eq. 2)
